The Origin of Chondrules and Refractory Inclusions in Chondritic Meteorites

Shu, Frank H.; Shang, Hsien; Gounelle, M.; Glassgold, A. E.; Lee, Typhoon

doi:10.1086/319018

Cited by 289 publications

(312 citation statements)

References 53 publications

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“…The energy released during the strongest event that we have detected is probably enough to bring chondrules to melting temperatures (∼2000 K), thus providing an alternative scenario to the protostellar flares in the fluctuating X-wind model proposed by Shu et al (2001), and the lightning or shock waves in the protoplanetary nebula. Flare events like the one we have observed could also explain the anomalous abundances of elemental isotopes in chondrules and the inclusions of the most pristine carbonaceous chondrites, and if they occur over several Myr, they might have important effects on the evolution of the primary atmospheres of Earth-like planets.…”

Section: Discussionmentioning

confidence: 67%

“…Some Ca, Al-rich inclusions (CAIs) in carbonaceous chondrites require formation temperatures as high as 1600 K. As for the chondrules, there is evidence of their having been brought to melting temperatures of ∼2000 K (Jones et al 2000;Shu et al 2001). A review of the models proposed for the chondrule and CAIs formation is given by Jones et al (2000).…”

Section: Effects Of Flares On Young Planetary Systemsmentioning

confidence: 99%

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The weak-line T Tauri star V410 Tau

Fernández¹,

Stelzer

Henden

et al. 2004

A&A

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Abstract. We show that V410 Tau, a weak-line T Tauri star, is a flaring star. This result comes from an intensive, coordinated monitoring campaign carried out in November 2001 at visible and X-ray wavelength ranges. It is confirmed by previous, isolated observations found in the literature. Flares tend to occur mainly around the star's minimum brightness, when the most active regions face us. We report on the strongest flare detected up to now on this star, for which we have obtained simultaneous visible Strömgren photometry and intermediate resolution spectroscopy. We derive decay times from 3 to 0.7 h at several wavelengths for the continuum in the 3600−5600 Å range. We estimate the energy involved in this and the other flares for which we have good time sampling, and conclude that the strongest event, at least, could have important consequences for the matter in the surroundings of the star. If similar events took place on the young Sun and lasted for several Myr, they could explain the anomalous abundances of elemental isotopes found in some meteorites. They could have also contributed to eliminate part of the primary atmospheres of the planet embryos and would have provided enough energy for the melting of solid iron-magnesium silicates, a process that may explain the presence of chondrules in chondritic meteorites. High resolution spectroscopy of the H α emission line in the quiescent states of V410 Tau enables us to study the variability of the broad component. We suggest that this component is related to microflaring activity, such as the one observed on more evolved, magnetically-active stars. The large velocities and the energy associated with this component support this hypothesis.

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Section: Discussionmentioning

confidence: 67%

Section: Effects Of Flares On Young Planetary Systemsmentioning

confidence: 99%

The weak-line T Tauri star V410 Tau

Fernández¹,

Stelzer

Henden

et al. 2004

A&A

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“…2 implies that the small grains have disappeared throughout the disk 1 . The X-wind mechanism (Shu et al 2001) may also be capable of adding some (processed) material on the surface of the disk. In that case, the composition of the surface layer as traced by the silicate feature is not representative of that of the bulk of the silicates.…”

Section: Discussionmentioning

confidence: 99%

Grain growth in the inner regions of Herbig Ae/Be star disks

Boekel

Waters

Dominik

et al. 2003

A&A

157

122

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Abstract. We present new mid-infrared spectroscopy of the emission from warm circumstellar dust grains in Herbig Ae/Be stars. Our survey significantly extends the sample that was studied by Bouwman et al. (2001). We find a correlation between the strength of the silicate feature and its shape. We interpret this as evidence for the removal of small (0.1 µm) grains from the disk surface while large (1-2 µm) grains persist. If the evolution of the grain size distribution is dominated by gravitational settling, large grains are expected to disappear first, on a timescale which is much shorter than the typical age of our programme stars. Our observations thus suggest a continuous replenishment of micron sized grains at the disk surface. If the grain replenishment is due to the dredge-up of dust from the disk interior, the mineralogy we observe is representative of the bulk composition of dust in these stars.

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“…If 26 Al is from an irradiation source, then this heat source must be supplied to the condensed matter making planets at least at a level of 26 Al/ 27 Al ∼ 10 −5 . [264]. There has been a major effort to seek an explanation for a large number of the short-lived nuclei by proto-solar cosmic rays impinging on dust or small rocks.…”

Section: Be and Irradiationmentioning

confidence: 99%

Short-lived nuclei in the early Solar System: Possible AGB sources

et al. 2006

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The abundances of short-lived radionuclides in the early solar system (ESS) are reviewed, as well as the methodology used in determining them. These results are compared with the inventory estimated for a uniform galactic production model. It is shown that, to within a factor of two, the observed abundances of 238 U, 235 U, 232 Th, 244 Pu, 182 Hf, 146 Sm, and 53 Mn are roughly compatible with long-term galactic nucleosynthesis. 129 I is an exception, with an ESS inventory much lower than expected from uniform production. The isotopes 107 Pd, 60 Fe, 41 Ca, 36 Cl, 26 Al, and 10 Be require late addition to the protosolar nebula. 10 Be is the product of energetic particle irradiation of the solar system as most probably is 36 Cl. Both of these nuclei appear to be present when 26 Al is absent. A late injection by a supernova (SN) cannot be responsible for most of the short-lived nuclei without excessively producing 53 Mn; it can however be the source of 53 Mn itself and possibly of 60 Fe. If a late SN injection is responsible for these two nuclei, then there remains the problem of the origin of 107 Pd and several other isotopes. Emphasis is given to an AGB star as a source of many of the nuclei, including 60 Fe; this possibility is explored with a new generation of stellar models. It is shown that if the dilution factor (i.e. the ratio of the contaminating mass to the solar parental cloud mass) is f 0 ∼ 4×10 −3 , a reasonable representation for many nuclei is obtained; this requires that ( 60 Fe/ 56 Fe) ESS ∼ 10 −7 to 2×10 −6 . The nuclei produced by an AGB source do not include 53 Mn, 10 Be or 36 Cl if it is very abundant. The role of irradiation is discussed with regard to 26 Al, 36 Cl and 41 Ca, and the estimates of bulk solar abundances of these isotopes are commented on. The conflict between various scenarios is emphasized as well as the current absence of an astrophysically plausible global interpretation for all the existing data. Examination of abundances for the actinides indicates that a quiescent interval of ∼ 10 8 years is required for actinide group production. This is needed in order to explain the data on 244 Pu and the new bounds on 247 Cm. Because this quiescent interval is not compatible with the 182 Hf data, a separate type of r-process event is needed for at least the actinides, distinct from the two types that have previously been identified. The apparent coincidence of the 129 I and trans-actinide time scales suggests that the last heavy r contribution was from an r-process that produced very heavy nuclei but without fission recycling so that the yields at Ba and below (including I) were governed by fission.

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The Origin of Chondrules and Refractory Inclusions in Chondritic Meteorites

Cited by 289 publications

References 53 publications

The weak-line T Tauri star V410 Tau

The weak-line T Tauri star V410 Tau

Grain growth in the inner regions of Herbig Ae/Be star disks

Short-lived nuclei in the early Solar System: Possible AGB sources

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